Evolution of High-energy Particle Distribution in Supernova Remnants. (arXiv:1911.08321v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Zeng_H/0/1/0/all/0/1">Houdun Zeng</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Xin_Y/0/1/0/all/0/1">Yuliang Xin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fu_Q/0/1/0/all/0/1">Qi Fu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_S/0/1/0/all/0/1">Siming Liu</a>
The spectra fits to a sample of 34 supernova remnants (Zeng et al., 2019) are
updated. $gamma$-ray spectra of 20 supernova remnants (SNRs) with a soft TeV
spectrum are further analyzed. We found that 17 of them can be fitted in the
hadronic scenario with a single power-law ion distribution with an index of
$sim$ 2.6, which is significantly softer than the ion distribution inferred
from $gamma$-ray observations of star-burst galaxies. If Galactic cosmic rays
are mostly produced by SNRs, this result suggests that SNRs in star-burst
galaxies may never reach the phase with a soft $gamma$-ray spectra or escape
of high-energy particles from SNRs before they reach this phase with a soft
$gamma$-ray spectrum dominates the contribution of SNRs to Galactic cosmic
rays.
The spectra fits to a sample of 34 supernova remnants (Zeng et al., 2019) are
updated. $gamma$-ray spectra of 20 supernova remnants (SNRs) with a soft TeV
spectrum are further analyzed. We found that 17 of them can be fitted in the
hadronic scenario with a single power-law ion distribution with an index of
$sim$ 2.6, which is significantly softer than the ion distribution inferred
from $gamma$-ray observations of star-burst galaxies. If Galactic cosmic rays
are mostly produced by SNRs, this result suggests that SNRs in star-burst
galaxies may never reach the phase with a soft $gamma$-ray spectra or escape
of high-energy particles from SNRs before they reach this phase with a soft
$gamma$-ray spectrum dominates the contribution of SNRs to Galactic cosmic
rays.
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